Gaia and Gould's Belt

Gaia and Gould’s Belt

Anthony Brown Leiden Observatory [email protected]

G The Gaia mission G Summary of the Gaia sky survey G Science performance G Data processing G Catalogue and archive access G Gaia impact on Gould’s Belt research

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.1/26 N ESA Cornerstone mission within Horizon 2000+ programme N Create large and highly accurate stereoscopic map of the Galaxy N Global astrometry concept successfully demonstrated by Hipparcos

N Launched on December 19 2013 with Soyuz-Fregat from Kourou N Orbit: vicinity of L2 N Mission duration 5 (+1) years

Image credit: Lund Observatory Image credits: NASA/JPL-Caltech/R. Hurt, ESA and ATG medialab Survey capabilities Simulated Gaia sky — Robin et al., arXiv:1202.0132 G Three simultaneous observing G < 20 mag modes 6.0 G Complete to G = 20( V = 20–22) 5.5 G Observing programme: autonomous on-board detection and unbiased 5.0 G 4.5 Quasi-regular time-sampling over 5 Grvs < 17 mag

years (∼ 70 observations) 4.0

G Angular resolution comparable to 3.5 HST 3.0 stars/sq degree 10 2.5

Number of objects log

2.0 N 1 billion stars to G = 20 Grvs < 12 mag N 106–107 galaxies 1.5 N 500 000 quasars 1.0 N 3 × 105 solar system bodies 0.5 N tens of thousands of exoplanets 0.0

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.4/26 Survey capabilities

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.5/26 Number of ﬁeld of view transits

Scan law simulations with AGISLab, image courtesy ESO/S. Brunier

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.6/26 Figure courtesy Xavier Luri, DPAC-CU2 and NASA/JPL-Caltech/R. Hurt Gaia astrometry

Parallax relative accuracy horizons (AV = 0.0) 25

M6V

M0V M0III K4V G2V K1III 20 B1V 10%

B0I 1% V 15 0.1%

5 101 102 103 104 105 106 Distance [pc]

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.8/26 Gaia astrometry

Parallax relative accuracy horizons (AV = 5.0) 25 M6V

M0V M0III 10% K4V G2V K1III 1% B1V B0I 20 0.1%

V 15

5 101 102 103 104 105 106 Distance [pc]

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For Galactic disk, with σ$ /$ < 0.3

Figure courtesy Franc¸ois Mignard

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.10/26 Gaia spectrophotometry

Photometer G Two channels: 330–680 nm (BP), 640–1000 nm (RP) G Low resolution (∼ 3–30 nm/pixel) prism spectra

G Allows derivation of AV , Teff, log g, [M/H], and [α/H] for brighter stars

sample sample 40 30 20 10 0 60 50 40 30 20 10 0

3.0 3.0

2.5 2.5 photons) photons) 3 3 2.0 2.0

1.5 1.5

1.0 1.0 BP counts (10 RP counts (10 0.5 0.5

0.0 0.0 400 500 680 900 640 700 800 9001000 λ (nm) λ (nm)

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.11/26 Gaia spectrophotometry

600 0.4 0.3 0

400 A Teff ε ε 0.2 200 0.1 0 0 8 10 12 14 16 18 20 8 10 12 14 16 18 20 G(mag) G(mag) 1.5 1.5

1 1 Logg [Fe/H] ε ε 0.5 0.5

0 0 8 10 12 14 16 18 20 8 10 12 14 16 18 20 G(mag) G(mag)

Example of stellar parametrization performance (in this case with SVM). From Liu et al., 2012, MNRAS 426, 2463

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.12/26 Gaia radial velocities N Slitless spectroscopy in Ca triplet region (847–874 nm) N λ/∆λ ∼ 11 000

] B0V 1

− B5V A0V A5V 15 F0V G0V G5V K0V K1IIIMP 10 K4V K1III

5 End-of-mission radial velocity error [km s

0 9 10 11 12 13 14 15 16 17 V [mag] ‘

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.13/26 Simulate your own

What G Background information on instruments and error modelling G Interpolation tables and formulae G Error variations on sky G Transformations from Johnson, Sloan systems to Gaia photometric system G Will be updated with more information on astrophysical parameter performances, other products from photometry and spectroscopy G Simulated Gaia catalogues (billion objects) will be made available through CDS

Where N Go to: www.rssd.esa.int/gaia, look for ‘Science Performance’ button I (or google for ‘Gaia science performance’) N Python implementation at: pypi.python.org/pypi/PyGaia

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.14/26 G Gaia data processing is a Pan-European cooperation I Over 1000 staff years effort since 2006 I Processing power spread over 6 centres Supported through DPAC I participating countries national funding October 2013 I Additional support from 450 members EC Marie Curie and ESF Including: BR CA DPCI DZ ESA IL DPCG US DPCC DPCT

DPCB DPCE Data release scenario

Figure by Franc¸ois Mignard

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.16/26 Data release scenario

G Assumes smooth commissioning and operations! G Each release updates the previous and contains signiﬁcant new additions G No proprietary period for DPAC

Launch December 19 2013 L+22M Positions + G magnitude (∼ all sky, single stars) • Includes more often scanned Ecliptic pole regions • Hundred Thousand Proper Motions (Hipparcos-Gaia, ∼ 50 µas/yr) L+28M radial velocities for bright stars, two-band photometry, and full astrometry (α, δ, $, µα∗, µδ) where available.

L+40M full astrometry, orbital solutions for short period binaries, (GBP − GRP), BP/RP Spectrophotometry and astrophysical parameters , radial velocities, RVS spectra L+65M Updates on previous release — including more sources, source classiﬁcations, multiple astrophysical parameters, variable star solutions and epoch photometry for them, solar system results End+3yr Everything

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.17/26 Gould’s Belt

www.handprint.com/ASTRO/galaxy.html#Gouldbelt

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.18/26 Gould’s Belt

Perrot & Grenier 2003

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.19/26 Hipparcos census of Gould’s Belt

G kinematic evidence for physical groups in 12 out of 22 ﬁelds G remaining 10 ﬁelds had unfavourable kinematics or distance for Hipparcos (e.g., Orion OB1) G Membership (previously Cepheus: Cep OB6

De Zeeuw, Hoogerwerf, de Bruijne, Brown, Blaauw, 1999

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.20/26 Gaia — Detailed 3D structure

Bouy et al 2014

G All of Gould’s Belt well within reach of accurate Gaia parallaxes I including low mass stars G Example: unravelling of 3D structure of Orion region I Hipparcos provided hints of foreground population in parallax distribution

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.21/26 Gaia — Detailed 3D structure

Brown, Walter, Blaauw 1998

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.22/26 Gaia — Kinematics at high accuracy

G Transverse motions to better than ∼ 0.5 km s−1 throughout Gould’s Belt G Radial velocities better than 2–5 km s−1 I down to K0V I complementary radial velocity surveys to match transverse motion accuracies G Precise membership of associations I new light on ‘boundaries’ of associations? G Resolving of internal motions I reconstruct birth conﬁguration of associations (Blaauw 1978) I kinematic ages G Tracing runaways to their origins I increase sample

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.23/26 Gaia — Astrophysics of Gould’s Belt

G Accurate calibration of stellar structure models I Gaia parallaxes, binary stars, asteroseismology I accurate ages for young stars (MS turn-on and turn-off) I study progression of star formation in Gould’s Belt G Chemical abundances (Gaia-ESO survey) I signatures of star formation by supernova triggering G Mapping the 3D distribution of ISM in and around Gould’s Belt Pecaut et al 2012 I Gaia combined with Planck, HI surveys, etc

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.24/26 Gaia — Astrophysics of Gould’s Belt

Lallement et al 2013

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.25/26 Stay tuned

Henk Musterman, Meppel

Gaia Survey Performance Data processing Catalogue and archive Gould’s Belt Groningen 2014.04.07 - p.26/26 Extra Material 3D position and velocity of star + satellite orbit, abberation, light bending, etc Direction Gaia–star Vector sun–star

Spacecraft attitude Data processing

Star position in Centroid stellar image telescope ﬁeld of view

Optical projection on detectors, location/orientation of detectors

1 Gaia spectroscopy N Slitless spectroscopy in Ca triplet region (847–874 nm) N λ/∆λ ∼ 11 000 20

] B0V 1

− B5V A0V A5V 15 F0V G0V G5V K0V K1IIIMP 10 K4V K1III

5 End-of-mission radial velocity error [km s

0 9 10 11 12 13 14 15 16 17 V [mag] ‘

Delivering the promise of Gaia Gaia limitations Groningen 2014.04.07 - p.29/26 Gaia spectroscopy

Stellar and interstellar parameters (conservative estimates) N Radial velocities V ≤ 17 ∼ 150 × 106 stars N Rotational velocities V ≤ 13 ∼ 5 × 106 N Atmospheric parameters V ≤ 13 ∼ 5 × 106 N Abundances V ≤ 12 ∼ 2 × 106 N Interstellar reddening V ≤ 13 ∼ 5 × 106

Diagnostics G Binarity/multiplicity, variability G ∼ 106 spectroscopic binaries G ∼ 105 eclipsing binaries (∼ 25% SB2 → masses)

G Long period classical Cepheids σvr < 7 km/s → 20–30 kpc

Delivering the promise of Gaia Gaia limitations Groningen 2014.04.07 - p.30/26 Reaching out to the general public

Efﬁcient access to a billion source catalogue Seamless inter-operation with other missions and surveys

Delivering Visualization to aid the the Promise Long term archive discovery process preservation in the context of of Gaia data re-use Your ideas here

• Give me all stars with a certain angular momentum N DPAC-CU9 has started work on the • I want to reprocess all Gaia data Gaia catalogue and archive and study the effects of systematic errors on σγ N Maximizing science depends on • Requested from my iDevice. . . archive that can deliver what you want I tell us how you want to access and use the Gaia data I feel free to go crazy. . . I think about possibilities in 2020!

Gaia Archive

Delivering the promise of Gaia Gaia limitations Groningen 2014.04.07 - p.32/26 Gaia data access use cases

G Provide your ideas through GREAT wiki pages I http://great.ast.cam.ac.uk/Greatwiki/GaiaDataAccess G Many ideas collected already G Reviewed and ranked according to I Urgency, generality, science impact, scale, expected frequency I ranking will be used to prioritize CU9 efforts G All of this is summarized in a publicly available document I http: //www.rssd.esa.int/SA/GAIA/docs/library/AB-026.htm

Please read this document and provide feedback (and keep ideas on use cases coming)!

Delivering the promise of Gaia Gaia limitations Groningen 2014.04.07 - p.33/26 −2 I Astrometric limit is ∼ 1 000 000 stars deg (without bright stars) −2 I Photometric limit is ∼ 750 000 stars deg (without bright stars) −2 I Spectroscopic limit is ∼ 36 000 stars deg (without bright stars) −2 I Up to ∼ 3 000 000 stars deg can be dealt with

I Detection depends on separation and magnitude difference

I On paper the limit is detection up to 200 mas I In reality, extended objects up to 700 mas are detected

I The paper limit is G = 5.7 mag (V = 6 mag is normally quoted) I The real limit is a bit better (and varies from CCD row to row) I Will extend to G ∼ 1.5 through on-board S/W change

G Crowding: incompleteness at high densities and faint magnitudes

G Spatial resolution: unresolved close binaries

G On-board processing: not optimised for extended objects

G Dynamic range: existence of a bright limit

Gaia’s ‘limitations’

G Sky-coverage non-uniformity I Average ∼ 70 observations over 5 years (∼ 20% dead time) I Varies over the sky between ∼ 50 and ∼ 130 (∼ 20% dead time)

Delivering the promise of Gaia Gaia limitations Groningen 2014.04.07 - p.34/26 I Detection depends on separation and magnitude difference

I On paper the limit is detection up to 200 mas I In reality, extended objects up to 700 mas are detected

I The paper limit is G = 5.7 mag (V = 6 mag is normally quoted) I The real limit is a bit better (and varies from CCD row to row) I Will extend to G ∼ 1.5 through on-board S/W change

G Spatial resolution: unresolved close binaries

G On-board processing: not optimised for extended objects

G Dynamic range: existence of a bright limit

Gaia’s ‘limitations’

Delivering the promise of Gaia Gaia limitations Groningen 2014.04.07 - p.35/26 Gaia’s ‘limitations’

Gaia’s view of R136, image courtesy Jos de Bruijne and Guido de Marchi Delivering the promise of Gaia Gaia limitations Groningen 2014.04.07 - p.36/26 Gaia’s ‘limitations’

Gaia’s view of R136, image courtesy Jos de Bruijne and Guido de Marchi

Delivering the promise of Gaia Gaia limitations Groningen 2014.04.07 - p.37/26 I On paper the limit is detection up to 200 mas I In reality, extended objects up to 700 mas are detected

I The paper limit is G = 5.7 mag (V = 6 mag is normally quoted) I The real limit is a bit better (and varies from CCD row to row) I Will extend to G ∼ 1.5 through on-board S/W change

G On-board processing: not optimised for extended objects

G Dynamic range: existence of a bright limit

Gaia’s ‘limitations’

Delivering the promise of Gaia Gaia limitations Groningen 2014.04.07 - p.38/26 I The paper limit is G = 5.7 mag (V = 6 mag is normally quoted) I The real limit is a bit better (and varies from CCD row to row) I Will extend to G ∼ 1.5 through on-board S/W change

G Dynamic range: existence of a bright limit

Gaia’s ‘limitations’

G Sky-coverage non-uniformity I Average ∼ 70 observations over 5 years (∼ 20% dead time) I Varies over the sky between ∼ 50 and ∼ 130 (∼ 20% dead time) G Crowding: incompleteness at high densities and faint magnitudes −2 I Astrometric limit is ∼ 1 000 000 stars deg (without bright stars) −2 I Photometric limit is ∼ 750 000 stars deg (without bright stars) −2 I Spectroscopic limit is ∼ 36 000 stars deg (without bright stars) −2 I Up to ∼ 3 000 000 stars deg can be dealt with G Spatial resolution: unresolved close binaries I Detection depends on separation and magnitude difference G On-board processing: not optimised for extended objects I On paper the limit is detection up to 200 mas I In reality, extended objects up to 700 mas are detected

Delivering the promise of Gaia Gaia limitations Groningen 2014.04.07 - p.39/26 Gaia’s ‘limitations’

Delivering the promise of Gaia Gaia limitations Groningen 2014.04.07 - p.40/26 Gaia’s ‘limitations’

Bright limit in G: 5.7 11

10 V 9

7 Bright limit of Gaia in

5 0 1 2 3 4 5 6 (V I) −

Delivering the promise of Gaia Gaia limitations Groningen 2014.04.07 - p.41/26